How many extragalactic stellar mass binary black holes will be detected by space gravitational-wave interferometers?
How many extragalactic stellar mass binary black holes will be detected by space gravitational-wave interferometers?
复制标题
空间引力波干涉仪将探测到多少个河外恒星质量双黑洞？
DOI：
10.1093/mnras/stac1561
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发表时间：
2022
影响因子：
4.8
通讯作者：
Kyutoku Koutarou
中科院分区：
文献类型：
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作者：
Seto Naoki;Kyutoku Koutarou
在GWTC-3的基础上，讨论了空间引力波干涉仪探测河外双星黑洞的前景，主要针对啁啾质量范围内的双星黑洞进行探测。特别是，我们直接将啁啾质量分布的62 BBH检测到目前为止，在高的意义。我们发现，由于减少了同动合并率和啁啾质量的加权平均，预期的检测数通常比由同一作者在GW 150914的报告后立即获得的结果小得多。对于丽莎，在啁啾质量范围内的总BBH探测估计为Ntot 2（T/4 yr）3/2（ρthr/10）−3，主要是近单色BBH（ρthr：探测阈值，T：观测周期）。天琴将有一个总的检测数Ntot类似于丽莎。同时，天琴有可能发现Nmer = 0.6（T/4 yr）7/4（ρthr/10）− 3BBH在观测期内发生合并。由于最佳频带的差异，用于合并BBH的这个数目比丽莎的数目大4-5倍。我们还研究了多个探测器联合操作的前景，发现并发观测比顺序观测更有利。
On the basis of GWTC-3, we discuss the detection prospect of extragalactic binary black holes (BBHs) by space gravitational-wave interferometers, mainly targeting BBHs in the range of chirp masses with abundant detections. In particular, we directly incorporate the chirp mass distribution of the 62 BBHs detected so far at high significance. We find that, due to the reduction of both the comoving merger rate and a weighted average of chirp masses, the expected detection numbers are generally much smaller than the results obtained by the same authors immediately after the report of GW150914. For LISA, the total BBH detections in the chirp mass range are estimated to beNtot∼ 2(T/4yr)3/2(ρthr/10)−3, dominated by nearly monochromatic BBHs (ρthr: the detection threshold,T: the observational period). TianQin will have a total detection numberNtotsimilar to LISA. Meanwhile, TianQin has potential to findNmer∼ 0.6(T/4yr)7/4(ρthr/10)−3BBHs that merge in the observational period. This number for merging BBHs is 4–5 times larger than that of LISA because of the difference of the optimal bands. We also investigate prospects for joint operations of multiple detectors, finding that concurrent observations will be more advantageous than sequential ones.